Search Results - "PAPICS, P"

Binary asteroseismic modelling: isochrone-cloud methodology and application to Kepler gravity mode pulsators by Johnston, C, Tkachenko, A, Aerts, C, Molenberghs, G, Bowman, D M, Pedersen, M G, Buysschaert, B, Pápics, P I

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THE INTERNAL ROTATION PROFILE OF THE B-TYPE STAR KIC 10526294 FROM FREQUENCY INVERSION OF ITS DIPOLE GRAVITY MODES by Triana, S. A., Moravveji, E., Pápics, P. I., Aerts, C., Kawaler, S. D., Christensen-Dalsgaard, J.

“…ABSTRACT The internal angular momentum distribution of a star is the key to determining its evolution. Fortunately, stellar internal rotation can be probed…”
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Kepler's first view of O-star variability: K2 data of five O stars in Campaign 0 as a proof of concept for O-star asteroseismology by Buysschaert, B., Aerts, C., Bloemen, S., Debosscher, J., Neiner, C., Briquet, M., Vos, J., Pápics, P. I., Manick, R., Schmid, V. S., Van Winckel, H., Tkachenko, A.

“…We present high-precision photometric light curves of five O-type stars observed with the refurbished Kepler satellite during its Campaign 0. For one of the…”
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The eccentric massive binary V380 Cyg: revised orbital elements and interpretation of the intrinsic variability of the primary component by Tkachenko, A., Degroote, P., Aerts, C., Pavlovski, K., Southworth, J., Pápics, P. I., Moravveji, E., Kolbas, V., Tsymbal, V., Debosscher, J., Clémer, K.

“…We present a detailed analysis and interpretation of the high-mass binary V380 Cyg, based on high-precision space photometry gathered with the Kepler space…”
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G 207-9 and LP 133-144: light-curve analysis and asteroseismology of two ZZ Ceti stars by Bognar, Zs, Paparo, M, Molnar, L, Papics, P I, Plachy, E, Verebelyi, E, Sodor, A

“…G 207-9 and LP 133-144 are two rarely observed ZZ Ceti stars located in the middle and close to the blue edge of the ZZ Ceti instability domain, respectively…”
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Stellar modelling of Spica, a high-mass spectroscopic binary with a β Cep variable primary component by Tkachenko, A., Matthews, J. M., Aerts, C., Pavlovski, K., Pápics, P. I., Zwintz, K., Cameron, C., Walker, G. A. H., Kuschnig, R., Degroote, P., Debosscher, J., Moravveji, E., Kolbas, V., Guenther, D. B., Moffat, A. F. J., Rowe, J. F., Rucinski, S. M., Sasselov, D., Weiss, W. W.

“…Binary stars provide a valuable test of stellar structure and evolution, because the masses of the individual stellar components can be derived with high…”
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DETECTION OF SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, AND STELLAR MODELS FOR θ CYG, THE BRIGHTEST STAR OBSERVED BY THE KEPLER MISSION by Guzik, J. A., Houdek, G., Chaplin, W. J., Smalley, B., Kurtz, D. W., Gilliland, R. L., Mullally, F., Rowe, J. F., Bryson, S. T., Still, M. D., Antoci, V., Appourchaux, T., Basu, S., Bedding, T. R., Benomar, O., Garcia, R. A., Huber, D., Kjeldsen, H., Latham, D. W., Metcalfe, T. S., Pápics, P. I., White, T. R., Aerts, C., Ballot, J., Boyajian, T. S., Briquet, M., Bruntt, H., Buchhave, L. A., Campante, T. L., Catanzaro, G., Christensen-Dalsgaard, J., Davies, G. R., Doğan, G., Dragomir, D., Doyle, A. P., Elsworth, Y., Frasca, A., Gaulme, P., Gruberbauer, M., Handberg, R., Hekker, S., Karoff, C., Lehmann, H., Mathias, P., Mathur, S., Miglio, A., Molenda- akowicz, J., Mosser, B., Murphy, S. J., Régulo, C., Ripepi, V., Salabert, D., Sousa, S. G., Stello, D., Uytterhoeven, K.

“…ABSTRACT θ Cygni is an F3 spectral type magnitude V = 4.48 main-sequence star that was the brightest star observed by the original Kepler spacecraft mission…”
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Spectroscopic survey of Kepler stars. ★ I. HERMES/Mercator observations of A- and F-type stars by Niemczura, E., Murphy, S. J., Smalley, B., Uytterhoeven, K., Pigulski, A., Lehmann, H., Bowman, D. M., Catanzaro, G., van Aarle, E., Bloemen, S., Briquet, M., De Cat, P., Drobek, D., Eyer, L., Gameiro, J. F. S., Gorlova, N., Kamiński, K., Lampens, P., Marcos-Arenal, P., Pápics, P. I., Vandenbussche, B., Van Winckel, H., Stȩślicki, M., Fagas, M.

“…The Kepler space mission provided near-continuous and high-precision photometry of about 207 000 stars, which can be used for asteroseismology. However, for…”
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Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades by White, T. R., Pope, B. J. S., Antoci, V., Pápics, P. I., Aerts, C., Gies, D. R., Gordon, K., Huber, D., Schaefer, G. H., Aigrain, S., Albrecht, S., Barclay, T., Barentsen, G., Beck, P. G., Bedding, T. R., Fredslund Andersen, M., Grundahl, F., Howell, S. B., Ireland, M. J., Murphy, S. J., Nielsen, M. B., Silva Aguirre, V., Tuthill, P. G.

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The puzzle of combination frequencies found in heat-driven pulsators by Papics, PI

“…Searching for combinations in the frequency spectra of variable stars is a commonly used method within the asteroseismological community, as harmonics and…”
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Wandering near the red edge: photometric observations of three cool ZZ Ceti stars by Bognár, Zs, Paparó, M, Sódor, Á, Jenei, D I, Kalup, Cs, Bertone, E, Chavez-Dagostino, M, Montgomery, M H, Győrffy, Á, Molnár, L, Ollé, H, Pápics, P I, Plachy, E, Verebélyi, E

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The discovery of a planetary candidate around the evolved low-mass Kepler giant star HD 175370 by Hrudkova, M, Hatzes, A, Karjalainen, R, Lehmann, H, Hekker, S, Hartmann, M, Tkachenko, A, Prins, S, Van Winckel, H, De Nutte, R, Dumortier, L, Fremat, Y, Hensberge, H, Jorissen, A, Lampens, P, Laverick, M, Lombaert, R, Papics, P I, Raskin, G, Sodor, A, Thoul, A, Van Eck, S, Waelkens, C

“…We report on the discovery of a planetary companion candidate with a minimum mass M sin I = 4.6 ± 1.0 M^sub Jupiter^ orbiting the K2 III giant star HD 175370…”
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Mass ratio from Doppler beaming and Rømer delay versus ellipsoidal modulation in the Kepler data of KOI-74 by Bloemen, S., Marsh, T. R., Degroote, P., Østensen, R. H., Pápics, P. I., Aerts, C., Koester, D., Gänsicke, B. T., Breedt, E., Lombaert, R., Pyrzas, S., Copperwheat, C. M., Exter, K., Raskin, G., Van Winckel, H., Prins, S., Pessemier, W., Frémat, Y., Hensberge, H., Jorissen, A., Van Eck, S.

“…We present a light-curve analysis and radial velocity study of KOI-74, an eclipsing A star + white dwarf binary with a 5.2-d orbit. Aside from new spectroscopy…”
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Modelling of σ Scorpii, a high-mass binary with a β Cep variable primary component by Tkachenko, A., Aerts, C., Pavlovski, K., Degroote, P., Pápics, P. I., Moravveji, E., Lehmann, H., Kolbas, V., Clémer, K.

“…High-mass binary stars are known to show an unexplained discrepancy between the dynamical masses of the individual components and those predicted by models. In…”
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More frequencies of KUV 02464+3239 by Bognár, Zs, Paparó, M., Már, A., Kerekes, Gy, Pápics, P., Molnár, L., Plachy, E., Sztankó, N., Bokor, E.

“…Preliminary results on KUV 02464+3239, a pulsating DA white dwarf are presented. Located near the red edge of the DAV instability strip, KUV 02464+3239 shows…”
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EMPIRICAL DETERMINATION OF CONVECTION PARAMETERS IN WHITE DWARFS. I. WHOLE EARTH TELESCOPE OBSERVATIONS OF EC14012-1446 by PROVENCAL, J. L, MONTGOMERY, M. H, BISCHOFF-KIM, A, STRICKLAND, W, CHANDLER, D, WALTER, B, WATSON, T. K, CASTANHEIRA, B, WANG, S, HANDLER, G, WOOD, M, VENNES, S, KANAAN, A, NEMETH, P, KEPLER, S. O, REED, M, NITTA, A, KLEINMAN, S. J, BROWN, T, KIM, S.-L, SULLIVAN, D, CHEN, W. P, YANG, M, THOMPSON, S. E, SHIH, C. Y, JIANG, X. J, SERGEEV, A. V, MAKSIM, A, JANULIS, R, BALIYAN, K. S, VATS, H. O, ZOLA, S, BARAN, A, WINIARSK, M, DALESSIO, J, OGLOZA, W, PAPARO, M, BOGNAR, Z, PAPICS, P, KILKENNY, D, SEFAKO, R, BUCKLEY, D, LOARING, N, KNIAZEV, A, SILVOTTI, R, SHIPMAN, H. L, GALLETI, S, NAGEL, T, VAUCLAIR, G, DOLEZ, N, FREMY, J. R, PEREZ, J, ALMENARA, J. M, FRAGA, L, CHILDERS, D, CLEMENS, J. C, ROSEN, R, HENRIQUE, P

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Spectroscopic frequencies of 4 CVn in 2010 and 2011 by Schmid, V.S., Themessl, N., Breger, M., Aerts, C., Beck, P.G., Castanheira, B.G., Fritz, V., Papics, P.I., Debosscher, J., Falcon, R.E.

“…Numerous high‐resolution spectra of the δ Scuti star 4 CVn were gathered at McDonald Observatory in Texas, USA. They were prepared for interpretation using…”
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Kepler 's first view of O-star variability: K2 data of five O stars in Campaign 0 as a proof of concept for O-star asteroseismology by Buysschaert, B., Aerts, C., Bloemen, S., Debosscher, J., Neiner, C., Briquet, M., Vos, J., Pápics, P. I., Manick, R., Schmid, V. S., Van Winckel, H., Tkachenko, A.

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The PLATO 2.0 mission by Rauer, H., Catala, C., Benz, W., Christensen-Dalsgaard, J., Deleuil, M., Goupil, M.-J., Janot-Pacheco, E., Santos, Ċ., Smith, A., Suárez, J.-C., Adibekyan, V., Alibert, Y., Almenara, J.-M., Barnes, S., Baudin, F., Bergemann, M., Bihain, G., Birch, A. C., Bonfils, X., Boisse, I., Bonomo, A. S., Borsa, F., Brandão, I. M., Brun, S., Burleigh, M., Cabrera, J., Charpinet, S., Church, R. P., Csizmadia, Sz, Cunha, M., Davies, M. B., Deeg, H. J., Díaz, R. F., Dreizler, S., Dreyer, C., Eggenberger, P., Eigmüller, P., Erikson, A., Farmer, R., Figueira, P., Fridlund, M., Giuffrida, G., da Silva, J. Gomes, Granzer, T., Grenfell, J. L., Günther, E., Haswell, C. A., Hébrard, G., Hekker, S., Heng, K., Johansen, A., Kislyakova, K. G., Kupka, F., Lammer, H., Marcos-Arenal, P., Marrese, P. M., Marques, J. P., Martins, J., Mathis, S., Mathur, S., Miglio, A., Montalban, J., Montalto, M., Moravveji, E., Morel, T., Mortier, A., Nascimbeni, V., Nelson, R. P., Nielsen, M. B., Noack, L., Norton, A. J., Ofir, A., Pápics, P., Quirrenbach, A., Raimondo, G., Rainer, M., Reese, D. R., Redmer, R., Reffert, S., Rojas-Ayala, B., Roxburgh, I. W., Salmon, S., Santerne, A., Schneider, J., Schou, J., Schuh, S., Schunker, H., Silva-Valio, A., Skillen, I., Snellen, I., Sozzetti, A., Strassmeier, K. G., Švanda, M., Tkachenko, A., Van Grootel, V., Vauclair, S. D., Ventura, P., Wagner, F. W., Wheatley, P. J., Zwintz, K.

“…PLATO 2.0 has recently been selected for ESA’s M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in…”
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Binary Asteroseismic Modelling: isochrone-cloud methodology and application to Kepler gravity-mode pulsators by Johnston, C, Tkachenko, A, Aerts, C, Molenberghs, G, Bowman, D. M, Pedersen, M. G, Buysschaert, B, Papics, P. I

“…The simultaneous presence of variability due to both pulsations and binarity is no rare phenomenon. Unfortunately, the complexities of dealing with even one of…”
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